{{Short description|Globular cluster in the constellation Apus}} {{Infobox globular cluster | name = IC 4499 | image = 260px | caption = IC 4499, as seen through the Hubble Space Telescope | credit = | epoch = J2000 | class = XI<ref name=seds/> | constellation = Apus | ra = {{RA|15|00|18.57}}<ref name=SIMBAD>{{cite simbad|title=IC 4499|access-date=20 February 2017}}</ref> | dec = {{DEC|-82|12|49.6}}<ref name=SIMBAD/> | dist_ly = {{convert|50,000|ly|pc|abbr=on|lk=on}}<ref name=seds/> | appmag_v =9.76<ref name=MWGC/> | size_v = 7.6{{prime}} × 7.6{{prime}}<ref name=seds/> | mass_msol = | mass_kg = | v_hb = | metal_fe = −1.53<ref name=MWGC>{{cite web|title=Catalog of Parameters for Milky Way Globular Clusters|url=http://physwww.mcmaster.ca/~harris/mwgc.dat|author1=William E. Harris|accessdate=3 February 2017}}</ref> | metal_z = | age = | notes = | names =GCl 30<ref name=SIMBAD/> }} '''IC 4499''' is a loose globular cluster in the constellation Apus. It is located in the medium-far galactic halo.<ref name=ferraro>{{cite journal |last1=Ferraro |first1=I. |last2=Ferraro |first2=F.R. |last3=Pecci |first3=F. Fusi |last4=Corsi |first4 = C.E. |last5=Buonanno |first5 = R. |date= August 1995 |title=Young globular clusters in the Milky Way: IC 4499 |journal=Monthly Notices of the Royal Astronomical Society |volume=275 |issue=4 |pages=1057–1076 |publisher=SAO/NASA ADS Astronomy Abstract Service |bibcode = 1995MNRAS.275.1057F |doi=10.1093/mnras/275.4.1057|doi-access=free }}</ref> Its apparent magnitude is 9.76,<ref name=seds>{{cite web|url =http://spider.seds.org/spider/MWGC/i4499.html|title = IC 4499 |publisher = Students for the Exploration and Development of Space |accessdate = 22 April 2012 |last = Frommert |first = Hartmut}}</ref> and was thought to be unusual because it appears to be 3–4 billion years younger than most other globular clusters in the Milky Way, as determined by metallicity measurements in 1995.<ref name="ferraro"/> However, this was contradicted in 2011 by results that yielded a much older age of 12 billion years.<ref name=Walker2011/>
As is typical for very old globular clusters, IC 4499 contains two generations of stars.<ref>[https://www.aanda.org/articles/aa/pdf/2018/10/aa33650-18.pdf IC 4499 revised: Spectro-photometric evidence of small light-element variations]</ref>
==References== {{Reflist|refs=
<ref name=Walker2011>{{citation | title=Constraints on the formation of the globular cluster IC 4499 from multiwavelength photometry | display-authors=1 | last1=Walker | first1=A. R. | last2=Kunder | first2=A. M. | last3=Andreuzzi | first3=G. | last4=di Cecco | first4=A. | last5=Stetson | first5=P. B. | last6=Monelli | first6=M. | last7=Cassisi | first7=S. | last8=Bono | first8=G. | last9=de Propris | first9=R. | last10=Dall'Ora | first10=M. | last11=Nemec | first11=J. M. | last12=Zoccali | first12=M. | journal=Monthly Notices of the Royal Astronomical Society | volume=415 | issue=1 | pages=643–654 | date=July 2011 | doi=10.1111/j.1365-2966.2011.18736.x | doi-access=free | bibcode=2011MNRAS.415..643W | arxiv=1103.4144 | s2cid=119180983 | postscript=. }}</ref>
}}
{{Apus}}
Category:Apus Category:Globular clusters 4499